Modeling Kepler's Supernova Remnant with VH-1

Weekly Updates:

9/7- I am continuing to work on the paper. The line of sight projections can now be output in NetCDF format to calculate velocities of points along the outer edge of the model remnant.
6/29- I am still attempting to check the values I am getting from the piece of code that completes the conversions from unitless to real values. The code does smoothly output the new values for density, velocity, and radius now. I am currently continuing to make sure that we are obtaining correct values from the conversions.
6/22-I have the piece of code that outputs the real unit values working and am currently trying to find things to compare to the values I obtain to make sure that the conversions are correct. Once this is done, I will be able to use the values I get to learn more about the model.
6/15-I have corrected the error in the code, which means models can now be run. Currently, I am working on adding real units to the values in the models.
6/7-I have determined that the bug casuing the features we are seeing is related to the conditions contained in the sweepx files. Once this is corrected, I will run simulations at a few various dynamical ages and determine the effect this has on the real values to be added into the model.

Most Recent Model Run:

Images of the most recent low res run (left) and high res run (right).

Previous Models:

The images below show results from the last three models before the high res run. The parameters of the middle one were used in the high res model.

Model Parameters:

Velocity Ratio

20

Density Ratio

2

Angle

30

Asymmetry Parameter A

0.5

Asymmetry Parameter B

7

Right:Volume rendered result from the lastest model run.

This model was run for 6000 cycles with files printed every 600 steps.

It was again observed that the areas that had broken through the bowshock displayed angular velocities at least comparable to the radial velocities at those points.

The following show rotations of the model around the Yand Z axis respectively, obtained by using the volume rendering tool in Ensight. The last animation shows the evolution of the model through time.

Model Parameters:

Velocity Ratio

20

Density Ratio

2

Angle

60

Asymmetry Parameter A

0.7

Asymmetry Parameter B

7

Right: Image colored by angular velocity component. The circled area corresponds to a region where the supernova blast wave has broken through the bowshock. In that region, we observe angular velocity that is comprable to, if not larger than, the radial velocity.

This model was run for 4000 cycles with files printed every 400 steps.

The following show rotations of the model around the X,Y,and Z axis respectively, obtained by using the volume rendering tool in Ensight. The last animation shows the evolution of the model through time.

Model Parameters:

Velocity Ratio

20

Density Ratio

2

Angle

45

Asymmetry Parameter A

0.7

Asymmetry Parameter B

7

Right: Rotation through Angle of the Model at the End Timestep

This model was run for 4000 cycles with files printed every 400 steps.

The following show rotations of the model around the X,Y,and Z axis respectively, obtained by using the volume rendering tool in Ensight. The last animation shows the evolution of the model through time.

Model Parameters:

Velocity Ratio

20

Density Ratio

2

Angle

30

Asymmetry Parameter A

0.7

Asymmetry Parameter B

7

Right: Rotation through Angle of the Model at the End Timestep

This model was run for 4000 cycles with files printed every 400 steps.

The following images show the remnant at different angles, like the animation above, as well as an animation that shows the evolution of the remnant through time from a single perspective.